Tracing the evolution of radiation-MHD simulations of solar and stellar atmospheres in the Lagrangrian frame

Abstract

Context: Radiation-MHD simulations have become a standard tool to investigate the physics of solar and stellar atmospheres. Aims: The aim of this paper to present a method that allows efficient and accurate analysis of flows in such simulations in the Lagrangian frame. Methods: This paper presents a method that allows the construction of pathlines given a seed point that can be chosen freely at any location and at any time during the simulation where the simulation state is stored. The method is based on passive tracer particles. Through injection of particles in expanding regions the occurrence of particle-free volumes is avoided, even in the case of strongly compressive flows. Results:The method was implemented in the solar and stellar atmosphere simulation code Bifrost. It is efficient and accurate. As examples I present an analysis of a gas parcel in the convection zone and a particle in the solar transition region.}

Accepted for publication in A&A

References in corpus (5)

• Magnetic flux emergence in granular convection: Radiative MHD simulations and observational signatures
• The origin of the reversed granulation in the solar photosphere
• On fibrils and field lines: The nature of H$\alpha$ fibrils in the solar chromosphere
• The cool surge following flux emergence in a radiation-MHD experiment
• On the plasma flow inside magnetic tornadoes on the Sun

Cited by in corpus (3)

• Structure and dynamics of the internetwork solar chromosphere: results of a small-scale dynamo simulation
• The formation and heating of chromospheric fibrils in a radiation-MHD simulation
• Non-Equilibrium Spectrum Formation Affecting Solar Irradiance